HD 172555

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HD 172555
Artist's concept of collision at HD 172555.jpg
An artist’s conception of a body about the size of the Moon slamming into a body the size of Mercury. As the bodies hit each other at speeds exceeding 10 km per second (about 22,400 mph), a huge flash of light is emitted, and their rocky surfaces are vaporized and melted, spraying hot matter everywhere.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pavo
Right ascension 18h 45m 26.9011s
Declination −64° 52′ 16.533″
Apparent magnitude (V) 4.8
Characteristics
Spectral type A5 IV/V[1]
Astrometry
Distance 95.34 ± 1.86 ly
(29.23 ± 0.57 pc)
Details
Mass 2.0[2] M
Luminosity 9.5[2] L
Temperature 8,000[1] K
Rotational velocity (v sin i) 175[3] km/s
Age ~12[2] Myr
Other designations
GC 25604, HIP 92024, SAO 254358.
Database references
SIMBAD data

HD 172555 is a white-hot A5V star located relatively close by, 95 light years from Earth in the direction of the constellation Pavo.[4] Spectrographic evidence indicates a relatively recent collision between two planet-sized bodies that destroyed the smaller of the two, which had been at least the size of Earth's moon, and severely damaged the larger one, which was at least the size of Mercury. Evidence of the collision was detected by NASA's Spitzer Space Telescope.[5]

Giant Hypervelocity Impact Debris[edit]

HD172555 was first recognized in the 1980s as being unusually bright in the mid-infrared by the IRAS sky survey. Follow-up ground based observations by Schütz et al. (2004) and the Spitzer Space Telescope, also in 2004 (Chen et al. 2006), confirmed the unusually strong nature of the infrared spectral emission from this system, much brighter than what would be emitted normally from the star's surface. As part of the Beta Pictoris moving group, HD172555 is coeval with that more famous system, approximately 12 million years old, and is the same kind of white-hot star as Beta Pic, about twice as massive as our Sun and about 9.5 times as luminous.[2] Comparison with current planetary formation theories, and with the very similar Beta Pic system, suggests that the HD172555 is in the early stages of terrestrial (rocky) planet formation. But what makes HD 172555 special is the presence of a large amount of unusual silicaceous material – amorphous silica and SiO gas – not the usual rocky materials, silicates like olivine and pyroxene, which make up much of the Earth as well.[6]

The material in the disk was analyzed in 2009 by Carey Lisse,[7] of the Johns Hopkins University Applied Physics Laboratory in Laurel, MD using the infrared spectrometer on board the Spitzer Space Telescope, and the results of the Deep Impact and STARDUST comet missions. Analysis of the atomic and mineral composition, dust temperature, and dust mass show a massive (about a Moon’s mass worth) amount of warm (about 340K) material similar to re-frozen lava (obsidian) and flash-frozen magma (tektite) as well as copious amounts of vaporized rock (silicon monoxide or SiO gas) and rubble (large dark pieces of dust) in a region at 5.8+/-0.6 AU from the HD172555 (at the edge of any terrestrial habitability zone, equivalent to a location in the inner part of the asteroid belt in our solar system). The material had to have been created in a hypervelocity impact between two large bodies; relative velocities at impacts less than 10 km/s would not transform the ubiquitous olivine and pyroxene into silica and SiO gas. Giant impacts at this speed typically destroy the incident body, and melt the entire surface of the impactee.

The implications for the detection of abundant amorphous silica and SiO gas are the following:

  • Massive hypervelocity impacts happen in young solar systems. There are a number of examples of such impacts in our own solar system (Hartmann & Vail 1986): Mercury’s high density; Venus’ retrograde spin; Earth’s Moon; Mars’ North/South hemispherical cratering anisotropy; Vesta’s igneous origin (Drake 2001); Uranus’ spin axis located near the plane of the ecliptic. Local geological evidence for widespread impact melting includes tektites found on Earth and glass beads found in lunarsoils (Warren 2008).
  • Rocky protoplanets, and possibly planets, exist in the HD172555 system, at about 12 Myr after its formation.
  • If the collision happened within the last few thousand years, there is likely a protoplanet in the HD172555 system with a liquid magma surface. This is not unexpected; a simple calculation of the gravitational binding energy of the Earth, shows that the energy released in assembling the Earth is about 10x the amount needed to melt it.

See also[edit]

References[edit]

  1. ^ a b Wyatt, M. C. et al. (July 2007), Steady State Evolution of Debris Disks around A Stars, The Astrophysical Journal 663 (1): 365–382, arXiv:astro-ph/0703608, Bibcode:2007ApJ...663..365W, doi:10.1086/518404 
  2. ^ a b c d Abundant Circumstellar Silica Dust and SiO Gas Created by a Giant Hypervelocity Collision in the ~12 Myr HD172555 System, by C. M. Lisse, C. H. Chen, M. C. Wyatt, A. Morlok, I. Song, G. Bryden, and P. Sheehan, The Astrophysical Journal, Volume 701, Number 2, August 20, 2009
  3. ^ Song, Inseok et al. (February 2001), Ages of A-Type Vega-like Stars from uvbyβ Photometry, The Astrophysical Journal 546 (1): 352–357, arXiv:astro-ph/0010102, Bibcode:2001ApJ...546..352S, doi:10.1086/318269 
  4. ^ When worlds collide Discover magazine, August 10, 2009
  5. ^ Two Planets Collide In Deep Space, Fox News, August 10, 2009
  6. ^ Clavin, Whitney (August 10, 2009). "Planet Smash-Up Sends Vaporized Rock, Hot Lava Flying". NASA. 
  7. ^ http://www.astro.umd.edu/~lisse/

External links[edit]

  • When worlds collide. Phil Plait, Discover website, Blogs / Bad Astronomy. August 10, 2009. NASA animation of what the collision may have looked like. Retrieved 2009-08-11

Further reading[edit]